| |
EI2GYB > ASTRO 30.08.21 11:31l 129 Lines 6467 Bytes #999 (0) @ WW
BID : 13889_EI2GYB
Read: GUEST
Subj: Teardrop star reveals hidden supernova doom
Path: IW8PGT<IZ3LSV<DB0ERF<DB0RES<PI8CDR<LU4ECL<ED1ZAC<GB7CIP<EI2GYB
Sent: 210830/0926Z 13889@EI2GYB.DGL.IRL.EURO BPQ6.0.22
_ _ _ _
/ \ ___| |_ _ __ ___ | \ | | _____ _____
/ _ \ / __| __| '__/ _ \ | \| |/ _ \ \ /\ / / __|
/ ___ \\__ \ |_| | | (_) | | |\ | __/\ V V /\__ \
/_/ \_\___/\__|_| \___/ |_| \_|\___| \_/\_/ |___/
Teardrop star reveals hidden supernova doom
Astronomers have made the rare sighting of two stars spiralling to
their doom by spotting the tell-tale signs of a teardrop-shaped star.
Astronomers have made the rare sighting of two stars spiralling to their
doom by spotting the tell-tale signs of a teardrop-shaped star.
The tragic shape is caused by a massive nearby white dwarf distorting the
star with its intense gravity, which will also be the catalyst for an
eventual supernova that will consume both.
Found by an international team of astronomers and astrophysicists led
by the University of Warwick, it is one of only very small number of
star systems that has been discovered that will one day see a white
dwarf star reignite its core.
New research published by the team today (12 July) in Nature Astronomy
confirms that the two stars are in the early stages of a spiral that will
likely end in a Type Ia supernova, a type that helps astronomers determine
how fast the universe is expanding.
This research received funding from the Deutsche Forschungsgemeinschaft
(DFG, German Research Foundation) and the Science and Technology
Facilities Council, part of UK Research and Innovation.
HD265435 is located roughly 1,500 light years away and comprises a hot
subdwarf star and a white dwarf star orbiting each other closely at a
rate of around 100 minutes.
White dwarfs are 'dead' stars that have burnt out all their fuel and
collapsed in on themselves, making them small but extremely dense.
A type Ia supernova is generally thought to occur when a white dwarf
star's core reignites, leading to a thermonuclear explosion.
There are two scenarios where this can happen. In the first, the white
dwarf gains enough mass to reach 1.4 times the mass of our Sun, known
as the Chandrasekhar limit.
HD265435 fits in the second scenario, in which the total mass of a
close stellar system of multiple stars is near or above this limit.
Only a handful of other star systems have been discovered that will
reach this threshold and result in a Type Ia supernova.
Lead author Dr Ingrid Pelisoli from the University of Warwick Department
of Physics, and formerly affiliated with the University of Potsdam,
explains: "We don't know exactly how these supernovae explode, but we
know it has to happen because we see it happening elsewhere in the universe.
"One way is if the white dwarf accretes enough mass from the hot
subdwarf, so as the two of them are orbiting each other and getting
closer, matter will start to escape the hot subdwarf and fall onto
the white dwarf. Another way is that because they are losing energy
to gravitational wave emissions, they will get closer until they merge.
Once the white dwarf gains enough mass from either method, it will go
supernova."
Using data from NASA's Transiting Exoplanet Survey Satellite (TESS),
the team were able to observe the hot subdwarf, but not the white dwarf
as the hot subdwarf is much brighter.
However, that brightness varies over time which suggested the star was
being distorted into a teardrop shape by a nearby massive object.
Using radial velocity and rotational velocity measurements from the
Palomar Observatory and the W. M. Keck Observatory, and by modelling
the massive object's effect on the hot subdwarf, the astronomers could
confirm that the hidden white dwarf is as heavy as our Sun, but just
slightly smaller than the Earth's radius.
Combined with the mass of the hot subdwarf, which is a little over
0.6 times the mass of our Sun, both stars have the mass needed to cause
a Type Ia supernova.
As the two stars are already close enough to begin spiralling closer
together, the white dwarf will inevitably go supernova in around 70
million years.
Theoretical models produced specifically for this study predict that
the hot subdwarf will contract to become a white dwarf star as well
before merging with its companion.
Type Ia supernovae are important for cosmology as 'standard candles'.
Their brightness is constant and of a specific type of light, which
means astronomers can compare what luminosity they should be with what
we observe on Earth, and from that work out how distant they are with a
good degree of accuracy.
By observing supernovae in distant galaxies, astronomers combine what
they know of how fast this galaxy is moving with our distance from the
supernova and calculate the expansion of the universe.
Dr Pelisoli adds: "The more we understand how supernovae work, the
better we can calibrate our standard candles.
This is very important at the moment because there's a discrepancy
between what we get from this kind of standard candle, and what we get
through other methods.
"The more we understand about how supernovae form, the better we can
understand whether this discrepancy we are seeing is because of new
physics that we're unaware of and not taking into account, or simply
because we're underestimating the uncertainties in those distances.
"There is another discrepancy between the estimated and observed galactic
supernovae rate, and the number of progenitors we see.
We can estimate how many supernovae are going to be in our galaxy
through observing many galaxies, or through what we know from stellar
evolution, and this number is consistent.
But if we look for objects that can become supernovae, we don't have enough.
This discovery was very useful to put an estimate of what a hot subdwarf
and white dwarf binaries can contribute.
It still doesn't seem to be a lot, none of the channels we observed seems
to be enough."
____ __ ____ ___ _ _ ____ ____ ____ ____
( __)( )(___ \ / __)( \/ )( _ \ ( _ \( _ \/ ___)
) _) )( / __/( (_ \ ) / ) _ ( ) _ ( ) _ (\___ \
(____)(__)(____) \___/(__/ (____/ (____/(____/(____/
PART OF THE DONEGAL PACKET RADIO NETWORK
Packet: EI2GYB@EI2GYB.DGL.IRL.EURO
Email: EI2GYB@GMAIL.COM
+------------------------------------------------------------------------------+
Read previous mail | Read next mail
| |
